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Detector Information

T-ReCS contains the same detector as Michelle . Some basic characteristics of the detectors are shown in the table below:

Entrance Windows

T-ReCS contains three entrance windows that are interchangeable in real time; the control software selects the window that is best for the specific observation and conditions.

Detector Information

T-ReCS contains the same detector as Michelle . Some basic characteristics of the detectors are shown in the table below:

Imaging

Basic characteristics of T-ReCS's imaging mode

T-ReCS is capable of imaging in the 8–26 micron range as follows:


  • Broad-band (N, Q) and Narrow-band Filter Imaging
  • Pixel size = 0.09" (fixed)
  • Field of view = 28.8"×21.6"
  • Number of filters: currently 20, capacity for 24
  • Occulting bar available for imaging (2" wide)

The principal T-ReCS imaging modes, plus the typical settings of five instrument components in each mode, are listed in the following table.

Sensitivity and Overheads

This section contains information on the sensitivity and performance of T-ReCS in its various observing modes. Go directly to:


Blocking Filters

The following table gives wavelength ranges of the order-sorting filters in NIRI that are used with the grisms. The Gemini identification number for each filter is recorded in data file headers.

Slits

The available slits are shown in the following table. The slit widths are given in pixels and arcsec projected on the sky. The spectral resolution is lower in a wider slit (see the grism table), even for point sources since under most atmospheric conditions the seeing wings of pointlike objects fill the wider slits. Note that for each f/6 slit width, 2 slits are available, one of which is offset from the optical axis and causes the spectrum to be shifted to shorter wavelengths on the array. Note also that the f/32 10 pixel wide slit and the f/6 2 pixel wide slit are the same slit.

Spectroscopy

Basic characteristics of T-ReCS's spectroscopy modes

T-ReCS is capable of spectroscopy with R~100 - 1000 in the 8–26 micron range as follows:

Imaging

Basic characteristics of T-ReCS's imaging mode

Taken from the current T-ReCS Intro page

Exposure times

The following five tables provide various exposure time limits. Constraints are due to a number of factors, more than one of which may need to be considered for a given NIRI configuration:

  • Minimum possible exposure time due to array electronics (Table 1)

  • Efficiency - ensuring that a much larger percentage of the time is spent exposing the array than reading it out (Table 2)

  • Time required for noise from fluctuations in the sky+telescope background to equal read noise (Table 3)

  • Maximum possible exposure time before array is saturated by background (Table 4)